As Fig. REF  clearly shows, there is no variability of the line profile or flux of the [Oi] 6300 Å or [Sii] 6730 Å forbidden lines in the timescale covered by our data. As was discussed in § 2.2, this is expected for the HVC, however if either of the other components were to originate from an MHD disk wind located in the innermost region of the disk, where accretion occurs, then we could expect to see some variability of that component on similar timescales as accretion. [1]} and [2]} show that the NLVC of the [Oi] 6300 Å line originates from the inner disk, but far enough from the central object that it should not be directly impacted by accretion (\(\,>\!0.5\,\) au, which was confirmed for RU Lup by [3]}), whereas the BC seems to trace a wind from closer in (between \(\sim 0.05\,\) au and \(\sim 0.5\,\) au from the central object). This latter component has velocities of \(\lesssim \!50\,\) km s\(^{-1}\)  and is therefore a LVC, unlike the BC of the [Oi] 6300 Å line of RU Lup, which is more blue-shifted. It is therefore evident that the broad component seen in the [Oi] 6300 Å line profile of RU Lup is not the same component as the broad low-velocity component (BLVC) described by [1]} and [2]} in their samples, but is likely an intermediate velocity component linked to the base of the jet [3]}. This star therefore lacks the BLVC which is linked to an MHD disk wind in the innermost part of the disk.
